Introduction To Modern Astronomy I

1. Introduction To Modern Astronomy I ASTR 111 – 003 Fall 2006 Lecture 03Sep. 18, 2006 Ch1: Astronomy and the Universe Ch2: Knowing the Heavens Ch3: Eclipses and the Motion of the Moon Ch4: Gravitation and the Waltz of the Planets Ch5: The Nature of Light Ch6: Optics and Telescope Introducing Astronomy (chap. 1-6) Planets and Moons (chap. 7-17) Note (added on Sep. 25, 2006): this ppt file contains the lecture note for the whole chap. 4. Section 4.1- 4.4 was taught on Sep. 18, 2006, and the other section 4.5 – 4.8 was taught on Sep. 25, 2006

2. Gravitation and the Waltz of the Planets Chapter Four

3. Guiding Questions • How did ancient astronomers explain the motions of the planets? • Why did Copernicus (1473-1543) think that the Earth and the other planets go around the Sun? • How did Tycho Brahe (1546-1601) attempt to test the ideas of Copernicus? • What paths do the planets follow as they move around the Sun? Johannes Kepler (1571-1630) • What did Galileo (1564-1642) see in his telescope that confirmed that the planets orbit the Sun? • What fundamental laws of nature explain the motions of objects on Earth as well as the motions of the planets? • Why don’t the planets fall into the Sun? • What keeps the same face of the Moon always pointed toward the Earth ?

4. Ancient Geocentric models • Ancient astronomers believed the Earth to be at the center of the universe, and the Earth is at rest • All the stars are fixed on the celestial sphere, rotating once a day • The Sun and Moon move slowly eastward with respect to the stars

5. Planetary Motion • Like the Sun and Moon, the planets usually move slowly eastward on the celestial sphere with respect to the background of stars • This eastward progress is called direct motion • Retrograde motion: but from time to time, the planets stop, and move westward for several weeks or months The Path of Mars in 2009-2010

6. Ptolemaic System: cycles on cycles • Ptolemaic system: each planet is assumed to move in a small cycle called an epicycle, whose center in turn moves in a large cycle, called a deferent, which is centered on the Earth • Both the epicycle and deferent rotates in the same direction ---- counter clock-wise

7. Ptolemaic System: cycles on cycles • When the planet is on the part of its epicycle nearest Earth, the motion of the planet along the epicycle is opposite to the motion of the epicycle along the deferent. The planet therefore appears to go backward in retrograde

8. Heliocentric Model by Copernicus • Heliocentric (Sun-centered) model: all the planets, including the Earth, revolve about the Sun • A heliocentric model simplifies the explanation of the retrograde motion of planets • Occam’s razor: simple explanations of phenomena are most likely to be correct Nicolaus Copernicus (1473 – 1543)

9. Heliocentric Model by Copernicus • Retrograde motion of a planet is caused by the Earth overtaking and passing the slow-moving planet • In the case of the Mars, it occurs during the period when the Sun, Earth and Mars are about aligned along a straight line

10. Planetary Configurations • Inferior planets: Mercury and Venus • Their orbits are smaller than the Earth • They are always observed near the Sun in the sky • Elongation: the angle between the Sun and a planet as viewed from Earth • Greatest Eastern Elongation: • Mercury or Venus visible after sunset • Called “evening star” • Greatest Western Elongation: • Mercury or Venus visible before sunrise • Called “morning star”

11. Planetary Configurations • Superior planets: Mars, Jupiter and Saturn • Their orbits are larger than the Earth • They can appear high in the sky at midnight, thus opposite the Sun with Earth in between • Conjunction: • The Sun and planet appear together in the celestial sphere • Opposition: • Earth is between Sun and planet • Planet is highest in the sky at midnight • Planet appears brightest because it is closest to the Earth

12. Synodic Period and Sidereal Period • Synodic period: the time that elapses between two consecutive identical configurations as seen from the Earth • e.g., from one opposition to the next for superior planets • e.g., from one greatest eastern elongation to the next for inferior planets • Sidereal period: true orbital period, the time it takes the planet to complete one full orbit of the Sun relative to the stars • Sidereal period is deduced from the observed synodic period

13. Heliocentric Model by Copernicus • Copernicus determined the sidereal period of planets • Copernicus also determined the distance of the planets from the Sun using trigonometry

14. Tycho Brahe’s Observations • Brahe’s observations measured the positions of stars and planets with unprecedented accuracy(about 1 arcmin) • The data obtained by Brahe put the heliocentric model on a solid foundation. Tycho Brahe (1546 – 1601)

15. Johannes Kepler • Using data collected by Tycho Brahe, Kepler deduced three laws of planetary motion, which are about • shape of orbits • speed of orbital motion • Relation between orbital size and orbital period Johannes Kepler (1571 – 1630)

16. Kepler’s First Law • Kepler’s first law: the orbit of a planet about the Sun is an ellipse, with the Sun at one focus • Semimajor axis: the average distance between the planet and the Sun • Assuming ellipse, Kepler found his theoretical calculations match precisely to Tycho’s observations.

17. Ellipse • Eccentricity e: the measure of the deviation from the perfect circle

18. Kepler’s Second Law • Kepler’s second law: a line joining a planet and the Sun sweeps out equal areas in equal interval of time • Perihelion: nearest the Sun; the planet moves fastest • Aphelion: farthest from the Sun; the planet moves slowest

19. Kepler’s Third Law • Kepler’s third law: the square of the sidereal period of a planet is directly proportional to the cube of the semimajor axis of the orbit P2 = a3 P = planet’s sidereal period, in years a = planet’s semimajor axis, in AU

20. Kepler’s Third Law • Kepler’s the law of planetary motion are a landmark in astronomy • They made it possible to calculate the motions of planets with better accuracy than any geocentric model ever had • They passed the test of Occam’s razor • They helped to justify the idea of heliocentric models

21. Introduction To Modern Astronomy II ASTR 111 – 003 Fall 2006 Lecture 04Sep. 25, 2006 Ch1: Astronomy and the Universe Ch2: Knowing the Heavens Ch3: Eclipses and the Motion of the Moon Ch4: Gravitation and the Waltz of the Planets (Exam 1 on Oct. 2: Chap.1 – Chap.4) Ch5: The Nature of Light Ch6: Optics and Telescope Introducing Astronomy (chap. 1-6) Planets and Moons (chap. 7-17) Note: this ppt file contains the lecture note for the whole chap. 4. Section 4.1- 4.4 was taught on Sep. 18, 2006, and other sections 4.5 – 4.8 will be covered today (Sep. 25, 2006)

22. Galileo’s Discoveries with Telescope • The invention of the telescope in the early 17th century led Galileo to new discoveries that permanently changed people’s view on the heavens. Galileo Galilei (1564 – 1642)

23. Galileo’s Discoveries: Phases of Venus α: apparent angular size of Venus as seen through telescope. Correction: the unit should be ’’ or arcsec instead of ° or degree • Venus exhibits phases like those of the Moon • The apparent size (α) is related to the planet’s phase • Venus appears larger at crescent phase • Venus appears smaller at gibbous phase

24. Galileo’s Discoveries: Phases of Venus • Heliocentric model provides a natural explanation for the phases of Venus • When Venus is on the same side of the Sun as the Earth, we see it a “new” phase and with a larger angular size • When Venus is on the opposite side of the Sun from the Earth, it appears full and has a small angular size

25. Galileo’s Discoveries: Phases of Venus • Galileo showed convincingly that the Ptolemaic geocentric model was wrong • To explain why Venus is never seen very far from the Sun, the Ptolemaic model had to assume that the deferents of Venus and of the Sun move together in lockstep, with the epicycle of Venus centered on a straight line between the Earth and the Sun • In this model, Venus was never on the opposite side of the Sun from the Earth, and so it could never have shown the gibbous phases that Galileo observed

26. Galileo’s Discoveries • Galileo discovered four moons, now called the Galilean satellites, orbiting Jupiter • Io, Europa, Ganymede and Callisto • The Earth is not at the center of all heavenly objects. • He also discovered • The Milky Way is not a featureless band of light, but “a mass of innumerable stars” • Mountains on the Moon • Sunspot on the Sun • Ring of Saturn

27. Isaac Newton • Isaac Newton, based on the insight into fundamental principles, introduced • three laws of motion • Law of Inertia • Law of Force • Law of Action and Reaction • the law of universal gravitation Isaac Newton (1642 -- 1727)

28. Newton First Law of Motion • First law of motion, or law of inertia: A body remains at rest, or moves in a straight line at a constant velocity, unless acted upon by a net outside force • Speed: a measure of how fast an object is moving • Velocity: the combination ofspeed and direction of motion • Acceleration: the rate at which velocity changes

29. Newton Second Law of Motion • Second law of motion, or law of force: The acceleration of an object is proportional to the net outside force acting on the object F = ma F = net outside force on an object m = mass of object a = acceleration of object • Mass: total amount of material in the object, an intrinsic value independent of gravitational environment; measured in Kg (Kilogram) • Weight: force of gravity that acts on a body; measured in Newton or Pound

30. Newton Third Law of Motion • Third law of motion, or law of action and reaction: Whenever one body exerts a force on a second body, the second body exerts an equal and opposite force on the first body

31. Newton’s Law of Universal Gravitation • Law of Universal Gravitation: Two bodies attract each other with a force that is directly proportional to the mass of each body and inversely proportional to the square of the distance between them F = gravitational force between two object m1 = mass of first object m2 = mass of second object r = distance between objects G = universal constant of gravitation: 6.67 × 10–11 newton • m2/kg2

32. Gravitation: Orbital Motions • Kepler’s three laws of planetary motion can be exactly derived from Newton’s law of universal gravitation • E.g., • closer to the Sun • stronger the gravitational force • faster the orbital speed • smaller the orbital period

33. Gravitation: Orbital Motions • The law of universal gravitation accounts for planets not falling into the Sun nor the Moon crashing into the Earth • Paths A, B, and C do not have enough horizontal velocity to escape Earth’s surface whereas Paths D, E, and F do. • Path E is where the horizontal velocity is exactly what is needed so its orbit matches the circular curve of the Earth

34. Gravitation: Orbital Motions • Based on his gravitational law, Newton found that the orbits of an object around the Sun could be any one of a family of curves called conic sections • Some comets are found to have hyperbolic orbits

35. Gravitation: Tidal Force • Tidal forces are differences in the gravitational pull at different points in an object • From the perspective of the center ball, it appears that the forces have pushed the 1-ball away and pulled the 3-ball toward the planets.

36. Gravitation: Tidal Force • The tidal force equals the Moon’s gravitational pull at the location minus the gravitational pull of the Moon at the center of the Earth • These tidal forces tend to deform the Earth into a non-spherical shape

37. Gravitation: Tidal Force • The positions of high tide caused by the Moon • Moon is at the upper local meridian (highest in the sky) • Moon is at the lower local meridian

38. Gravitation: Tidal Force • Spring tide • the highest tide, when the tidal effects of the Sun and Moon reinforce each other • Happens at either new moon or full moon • Neap tide • the smallest tide, when the tidal effects of the Sun and Moon partially cancelled each other • Happens at either first quarter or third quarter

39. Final Notes on Chap. 4 • There are 8 sections. And every section is covered • There are 4 boxes. None of them is covered in the lecture. You are encouraged to study them on your own